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Multiple star system in the constellation Virgo From Wikipedia, the free encyclopedia
HD 126614 is a trinary star[14] system in the equatorial constellation of Virgo. The primary member, designated component A, is host to an exoplanetary companion. With an apparent visual magnitude of 8.81,[7] it is too faint to be seen with the naked eye. The system is located at a distance of 239 light years from the Sun based on parallax measurements,[1] but is drifting closer with a radial velocity of −33 km/s.[8]
Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Virgo |
HD 126614 A | |
Right ascension | 14h 26m 48.279494s[1] |
Declination | −05° 10′ 40.01306″[1] |
Apparent magnitude (V) | 8.81±0.03[2] |
LP 680-57 | |
Right ascension | 14h 26m 45.836397s[3] |
Declination | −05° 10′ 19.427938″[3] |
Apparent magnitude (V) | 16.68±0.20[2] |
Characteristics | |
Spectral type | G8IV[4] + M[5] + M5.5V[6] |
Apparent magnitude (B) | 9.620[7] |
Apparent magnitude (J) | 7.470±0.021[7] |
Apparent magnitude (H) | 7.160±0.042[7] |
Apparent magnitude (K) | 7.060±0.036[7] |
B−V color index | 0.810±0.004[7] |
Astrometry | |
HD 126614 A | |
Radial velocity (Rv) | −32.897±0.0042[8] km/s |
Proper motion (μ) | RA: −149.760±0.023 mas/yr[1] Dec.: −145.837±0.018 mas/yr[1] |
Parallax (π) | 13.6633 ± 0.0166 mas[1] |
Distance | 238.7 ± 0.3 ly (73.19 ± 0.09 pc) |
Absolute magnitude (MV) | 4.52[7] |
LP 680-57 | |
Radial velocity (Rv) | −29.45±5.52[3] km/s |
Proper motion (μ) | RA: −147.861±0.038 mas/yr[3] Dec.: −149.118±0.034 mas/yr[3] |
Parallax (π) | 13.6050 ± 0.0316 mas[3] |
Distance | 239.7 ± 0.6 ly (73.5 ± 0.2 pc) |
Absolute magnitude (MV) | 12.02[5] |
Orbit[9] | |
Companion | HD 126614 B |
Period (P) | 59.979+4.696 −5.059 yr |
Semi-major axis (a) | 15.229+0.984 −1.094 AU |
Eccentricity (e) | 0.056+0.017 −0.018 |
Inclination (i) | 16.294+0.881 −0.771° |
Longitude of the node (Ω) | 284.664+2.600 −3.304° |
Periastron epoch (T) | 2450124.747+26.090 −28.486 |
Argument of periastron (ω) (secondary) | 240.567+30.578 −43.150° |
Semi-amplitude (K1) (primary) | 0.167573+0.012902 −0.011124 km/s |
Details | |
HD 126614 A | |
Mass | 1.145±0.03[5] M☉ |
Radius | 1.09±0.06[5] R☉ |
Luminosity | 1.21±0.19[5] L☉ |
Surface gravity (log g) | 4.39±0.08[5] cgs |
Temperature | 5,585±44[5] K |
Metallicity | +0.56±0.04[5] |
Rotation | ~99 days[5] |
Rotational velocity (v sin i) | 2.0±0.5[5] km/s |
Age | 7.2±2.0[5] Gyr |
HD 126614 B | |
Mass | 81.128+7.778 −7.922[9] MJup |
LP 680-57 | |
Mass | 0.32[10][11] M☉ |
Radius | 0.32[10][11] R☉ |
Luminosity | 0.0106[10] L☉ |
Surface gravity (log g) | 4.93[10] cgs |
Temperature | 3,275[10][11] K |
Metallicity [Fe/H] | +0.46[6] dex |
Age | 3.6 – 6.0[6] Gyr |
Other designations | |
HD 126614 AB: BD–04°3690, HD 126614, HIP 70623, SAO 139932, PPM 197558, G 124-40, LTT 5698, NLTT 37355[12] | |
LP 680-57: LP 680-57, NLTT 37349[13] | |
Database references | |
SIMBAD | A |
C | |
Exoplanet Archive | data |
The primary is a late G-type star with a stellar classification of G8IV.[4] It is a super metal-rich star; among the most metal-rich stars currently known.[15] This is most likely an evolving subgiant star, but the very high metallicity makes comparisons to standard spectral types difficult.[16]
In 2010, a close stellar companion was resolved and designated component C. This object is a faint red dwarf at an angular separation of 0.5″, which corresponds to a projected physical separation of ~ 36 AU.[16] More recent observations using radial velocity and astrometry have refined the parameters of HD 126614 C. It has an orbital period of about 60 years, with a smaller semi-major axis of 15 AU and a very low mass of 81.1 MJ.[9] This mass is very near the mass limit allowed for hydrogen fusion.
The outer companion, designated LP 680-57, was first reported in 1960 with the W. J. Luyten proper motion catalog.[17] It is a magnitude 17.0 red dwarf with a class of M5.5,[6] located at an angular separation of 41.90″ from the primary along a position angle of 299°, as of 2015.[17] They have a physical projected separation of 3,040 AU.[6] The common proper motion of the system has been confirmed, indicating that they are gravitationally bound.[16] Many multiple star catalogues still refer to this companion as component B, as it was known prior to the discovery of the closer companion.[17]
A Doppler search for giant planets begun in 1997 at the Keck Observatory provided an 11 year baseline for detecting periodicity in the primary star's radial velocity data. In 2010, a Jovian companion was announced with an orbital period of 3.41 years.[5] In 2022, the inclination and true mass of HD 126614 Ab were measured via astrometry.[9]
Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (years) |
Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
b | 0.339+0.204 −0.019 MJ |
2.249+0.088 −0.096 |
3.442+0.016 −0.017 |
0.548+0.063 −0.062 |
97.477+35.340 −37.849° |
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